Lecture Outlines Chapter 9 Astronomy Today 7th Edition Chaisson/McMillan
Chapter 9 Venus
Units of Chapter 9 9.1 Orbital Properties 9.2 Physical Properties 9.3 Long-Distance Observations of Venus 9.4 The Surface of Venus 9.5 The Atmosphere of Venus 9.6 Venus s Magnetic Field and Internal Structure
9.1 Orbital Properties Venus is much brighter than Mercury, and can be farther from the Sun Called morning or evening star, as it is still tied to Sun Brightest object in the sky, after Sun and Moon
9.1 Orbital Properties Apparent brightness of Venus varies, due to changes in phase and distance from Earth
9.2 Physical Properties Radius: 6000 km Mass: 4.9 x 10 24 kg Density: 5200 kg/m 3 Rotation period: 243 days, retrograde
9.2 Physical Properties Slow, retrograde rotation of Venus results in large difference between solar day (117 Earth days) and sidereal day (243 Earth days); note that the solar day is a large fraction of the year, and the sidereal day is even longer than the year.
9.3 Long-Distance Observations of Venus Dense atmosphere and thick clouds make surface impossible to see Surface temperature is about 730 K hotter than Mercury!
9.3 Long-Distance Observations of Venus Even probes flying near Venus, using ultraviolet or infrared, can see only a little deeper into the clouds
9.4 The Surface of Venus Surface is relatively smooth Two continent-like features: Ishtar Terra and Aphrodite Terra No plate tectonics Mountains, a few craters, many volcanoes and large lava flows
9.4 The Surface of Venus Surface mosaics of Venus
9.4 The Surface of Venus Surface maps of Venus, with Earth comparison
9.4 The Surface of Venus Ishtar Terra is one of two continent-sized features on the surface of Venus
9.4 The Surface of Venus The other is Aphrodite Terra
9.4 The Surface of Venus Lava has flowed from cracks on the surface
9.4 The Surface of Venus Volcanoes on Venus; most are shield volcanoes
9.4 The Surface of Venus Other volcanic features include lava domes and coronas
9.4 The Surface of Venus Impact craters on Venus, the largest named after Margaret Mead
9.4 The Surface of Venus Photographs of the surface, from the Venera landers
9.5 The Atmosphere of Venus Venus s atmosphere is very dense Solid cloud bank 50 70 km above surface Atmosphere is mostly carbon dioxide; clouds are sulfuric acid
9.5 The Atmosphere of Venus Upper atmosphere of Venus has high winds, but atmosphere near surface is almost calm
9.5 The Atmosphere of Venus There are also permanent vortices at the poles; the origin of the double-lobed structure is a mystery
9.5 The Atmosphere of Venus Venus is the victim of a runaway greenhouse effect just kept getting hotter and hotter as infrared radiation was reabsorbed
9.6 Venus s Magnetic Field and Internal Structure No magnetic field, probably because rotation is so slow No evidence for plate tectonics Venus resembles a young Earth (1 billion years) no asthenosphere, thin crust
Summary of Chapter 9 Venus is never too far from Sun and is the brightest object in the sky (after the Sun and Moon) Atmosphere very dense, mostly carbon dioxide Surface hidden by cloud cover Surface temperature 730 K Rotation slow and retrograde
Summary of Chapter 9 (cont.) Many lava domes and shield volcanoes Venus is comparable to Earth in mass and radius Large amount of carbon dioxide in atmosphere, and closeness to Sun, led to runaway greenhouse effect and very hot surface